Cosmic-ray production rates of He-, Ne- and Ar-isotopes in H-chondrites based on 36Cl-36Ar-ages

Details Cosmic-ray production rates of He-, Ne- and Ar-isotopes in H-chondrites based on 36Cl-36Ar-ages Cosmic-ray production rates of He-, Ne- and Ar-isotopes in H-chondrites based on 36Cl-36Ar-ages

Jul 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001m%26ps...36..963l&link_type=abstract

Meteoritics & Planetary Science, vol. 36, no. 6, p. 963-973

Computer Science

8

Scientific paper

We present the concentrations and isotopic compositions of He, Ne, and Ar for non-magnetic fractions and bulk samples of 17 H-chondrites which were recently investigated for their 36Cl-36Ar cosmic-ray exposure ages (Graf et al., 2001). All selected meteorites are observed falls with cosmic-ray exposure ages close to the 7 Ma peak. The rare gas data are consistent with 10Be and 36Cl production rates in the metal phase. Remarkably, only one out of the 17 H-chondrites, Bath, shows clear indications for a complex exposure history. Based on rare gas concentrations and 36Cl-36Ar exposure ages, 21Ne production rates as a function of 22Ne/21Ne and a mean 38Ar production rate are determined. The results confirm model calculations which predict that the relationship between 21Ne production rates and 22Ne/21Ne is ambiguous for high shielding. Besides the mean 38Ar production rate we also give production rate ratios P(38Ar from Ca) / P(38Ar from Fe). They vary between 10 and 77, showing no significant correlation with 38Ar-concentrations or 22Ne/21Ne. By investigating the metal-separates, Graf et al. (2001) found significant 3He deficits for six out of the 17 meteorites. For the non-magnetic fractions and bulk samples investigated here the data points in a 3He/21Ne versus 22Ne/21Ne diagram plot in the area defined by most of the H-chondrites. This means that 3He deficits in the metal phase are much more pronounced than in silicate minerals and we will argue that 3H diffusive losses in meteorites should be the rule rather than the exception. The 21Ne exposure ages, calculated on the basis of modeled 21Ne production rates, confirm the assumption by Graf et al. (2001) that the H5-chondrites with low 3He/38Ar in the metal formed in a separate event than those with normal 3He/38Ar ratios. The data can best be interpreted by assuming that the prominent 7 Ma exposure age peak of the H-chondrites is due to at least two events about 7.0 and 7.6 Ma ago.

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